Weak Emission Lines in the Wings of Solar H and K

Details Weak Emission Lines in the Wings of Solar H and K Weak Emission Lines in the Wings of Solar H and K

Jun 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011soph..270..485l&link_type=abstract

Solar Physics, Volume 270, Issue 2, pp.485-491

Physics

Solar Spectrum, Emission Lines, Chromosphere, Photosphere, Cycle Variability

Scientific paper

The rare-earth ions cerium ii, lanthanum ii, dysprosium ii, and additionally zirconium ii and iron ii, are seen as weak emission features in the wings of the solar Ca ii H and K lines. The strength of these emission lines increases on the disk toward the limb. We provide recent high-resolution observations at disk center and at the limb. The identity of the weak lines is re-worked. We point out the unique role of eclipse spectra in distinguishing between the photospheric and chromospheric origins of emission lines. It is then demonstrated from our full disk (Sun-as-a-Star) and center disk archives, 1974 - 2010, that no activity cycle related signal is evident (save for the H and K lines themselves).

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